On heating of solar active regions by magnetic energy dissipation

Solar Physics ◽  
1985 ◽  
Vol 95 (1) ◽  
pp. 69-72 ◽  
Author(s):  
Mukul Kumar ◽  
Udit Narain
Keyword(s):  
Energy Dissipation ◽  
Magnetic Energy ◽  
Active Regions ◽  
Solar Active Regions

Numerical Short-Term Solar Activity Forecasting

2017 ◽  
Vol 13 (S335) ◽  
pp. 243-249 ◽  
Author(s):  
Huaning Wang ◽  
Yihua Yan ◽  
Han He ◽  
Xin Huang ◽  
Xinghua Dai ◽  
...  
Keyword(s):  
Solar Activity ◽  
Magnetic Fields ◽  
Solar Atmosphere ◽  
Magnetic Energy ◽  
Three Dimensional ◽  
Active Regions ◽  
Short Term ◽  
Solar Active Regions ◽  
Solar Eruptions ◽  
Dimensional Reconstruction

AbstractIt is well known that the energy for solar eruptions comes from magnetic fields in solar active regions. Magnetic energy storage and dissipation are regarded as important physical processes in the solar corona. With incomplete theoretical modeling for eruptions in the solar atmosphere, activity forecasting is mainly supported with statistical models. Solar observations with high temporal and spatial resolution continuously from space well describe the evolution of activities in the solar atmosphere, and combined with three dimensional reconstruction of solar magnetic fields, makes numerical short-term (within hours to days) solar activity forecasting possible. In the current report, we propose the erupting frequency and main attack direction of solar eruptions as new forecasts and present the prospects for numerical short-term solar activity forecasting based on the magnetic topological framework in solar active regions.

scholarly journals Magnetic Field Topology in Solar Active Regions

1993 ◽  
Vol 141 ◽  
pp. 435-438
Author(s):  
N. Seehafer
Keyword(s):  
Magnetic Field ◽  
Magnetic Energy ◽  
Mean Field ◽  
Active Regions ◽  
Field Configuration ◽  
Relaxation Processes ◽  
Magnetic Field Topology ◽  
Solar Active Regions ◽  
Global Magnetic Field ◽  
Slow Evolution

AbstractIn solar active regions, over extended periods of time the plasma-magnetic field configuration evolves quasistatically through a sequence of nearly force-free equilibrium states. This evolution may be understood as the continual distortion of an existing equilibrium by wavelike disturbances propagating upward from the photosphere and subsequent fast relaxation to a new, neighbouring equilibrium. In the present paper the build-up of magnetic energy, which is presumably necessary for flares and other explosive events, during a quasistatic evolution is considered. If during the slow evolution the magnetic energy is increased, then the relaxation processes represent inverse cascades of energy. We study the conditions under which such cascades are possible within the framework of mean-field MHD. In contrast to the convection zone, where the dynamo for the global magnetic field of the Sun works, the solar atmosphere is convectively stable and the first order smoothing approximation justified. It turns out then that current helicity (B.∇ × B) is an important quantity decisive for whether magnetic energy can be built up.

scholarly journals STATISTICAL STUDY OF FREE MAGNETIC ENERGY AND FLARE PRODUCTIVITY OF SOLAR ACTIVE REGIONS

2014 ◽  
Vol 788 (2) ◽  
pp. 150 ◽  
Author(s):  
J. T. Su ◽  
J. Jing ◽  
S. Wang ◽  
T. Wiegelmann ◽  
H. M. Wang
Keyword(s):  
Statistical Study ◽  
Magnetic Energy ◽  
Active Regions ◽  
Solar Active Regions ◽  
Free Magnetic Energy ◽  
Flare Productivity

scholarly journals THE MAGNETIC ENERGY-HELICITY DIAGRAM OF SOLAR ACTIVE REGIONS

2012 ◽  
Vol 759 (1) ◽  
pp. L4 ◽  
Author(s):  
Kostas Tziotziou ◽  
Manolis K. Georgoulis ◽  
Nour-Eddine Raouafi
Keyword(s):  
Magnetic Energy ◽  
Active Regions ◽  
Solar Active Regions

scholarly journals MAGNETIC ENERGY SPECTRA IN SOLAR ACTIVE REGIONS

2010 ◽  
Vol 720 (1) ◽  
pp. 717-722 ◽  
Author(s):  
Valentyna Abramenko ◽  
Vasyl Yurchyshyn
Keyword(s):  
Magnetic Energy ◽  
Active Regions ◽  
Energy Spectra ◽  
Solar Active Regions
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